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Chandra X-Ray Observatory

CXC

1. Comparison of RGS Model for 1E0102.2-7219 to the HETG data 2. BI CCD CTI Correction for ACIS

Paul Plucinsky, Dan Dewey, & Joseph DePasquale
1

Paul Plucinsky

EPIC Cal October 2006


Chandra X-Ray Observatory
Gratuitous Pretty Pictures of E0102
S3 Summed Data ~100 ks

CXC

RGS Spectrum (Pollock 2006)

Objective: develop a spectral model which can be used by RGS, HETG, EPIC & ACIS, etc.
Paul Plucinsky 2

EPIC Cal October 2006


Chandra X-Ray Observatory
What's New Since the Iceland 2006 Meeting?

CXC

· Pollock's model based on the RGS data has been used by Dan
Dewy of the HETG team to compare to the HETG data · Dan adopted the RGS spectral model, including the normalizations · Dan developed a spatial model for the structure of the remnant · He created simulated datasets to compare the against the MEG and HEG data from the Chandra HETG

The overall agreement is encouraging !!!

· Good agreement on the bright lines, some disagreement on the
weaker lines

All of the following work has been done by Dan, many thanks !!!
Paul Plucinsky 3

EPIC Cal October 2006


Chandra X-Ray Observatory
Dewey Spatial and Spectral Model

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Paul Plucinsky

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EPIC Cal October 2006


Chandra X-Ray Observatory
MEG minus 1st order

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MgXI
Simulation

NeX NeIX

OVIII

OVII

Comparison

KS test

Paul Plucinsky

5

EPIC Cal October 2006


Chandra X-Ray Observatory
MEG plus 1st order

CXC

MgXI
Simulation

NeX NeIX

OVIII

OVII

Comparison

KS test

Paul Plucinsky

6

EPIC Cal October 2006


Chandra X-Ray Observatory
HEG minus 1st order

CXC

MgXI
Simulation

NeX NeIX

Comparison

KS test

Paul Plucinsky

7

EPIC Cal October 2006


Chandra X-Ray Observatory
HEG plus 1st order

CXC

MgXI
Simulation

NeX

NeIX

Comparison

KS test

Paul Plucinsky

8

EPIC Cal October 2006


Chandra X-Ray Observatory
Where Do We Go From Here ?

CXC

· Dewey analysis needs to be updated with latest response files for
HRMA/ACIS/HETG · Line-based analysis needs to be updated with the latest response files for HRMA/HETG/ACIS · RGS data need to be re-analyzed with new background model for RGS · RGS and HETG teams agree on a model well before the IACHEC meeting in California · ACIS, MOS, and pn use the new model to fit the CCD spectra

Paul Plucinsky

9

EPIC Cal October 2006


Chandra X-Ray Observatory
2. CTI Correction in CIAO for S3 and S1

CXC

· Penn State CTI corrector available since 2001 · CXC response products for S1 and S3 used a position-dependent
gain correction which recovers the true values of the PHs but does not improve the spectral resolution · S3 and S1 data will now be CTI-corrected in the events files provided to GOs · All TEN CCDs will be CTI-corrected as of CIAO and CALDB release in December 2006 · small, but significant improvement in spectral resolution and QE uniformity

Paul Plucinsky

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EPIC Cal October 2006


Chandra X-Ray Observatory
BI CTI correction: PH vs. Row #
Current CALDB: no CTI correction Prototype CALDB: CTI correction

CXC

Paul Plucinsky

11

EPIC Cal October 2006


Chandra X-Ray Observatory
BI CTI correction: PH vs. Row #

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Paul Plucinsky

12

EPIC Cal October 2006


Chandra X-Ray Observatory
S3 CTI correction: Mn-K at the Aimpoint
No CTI correction: FWHM~162 eV

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With CTI correction: FWHM~151 eV

Paul Plucinsky

13

EPIC Cal October 2006


Chandra X-Ray Observatory
S3 CTI correction: Mn-K at the Top
No CTI correction: FWHM~182 eV

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With CTI correction: FWHM~157 eV

Paul Plucinsky

14

EPIC Cal October 2006


Chandra X-Ray Observatory
Current CALDB No CTI correction: E0102 on S3 Red Chi= 1.44

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Paul Plucinsky

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EPIC Cal October 2006


Chandra X-Ray Observatory
BI CTI correction: E0102 on S3 Red Chi= 1.10

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Paul Plucinsky

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EPIC Cal October 2006


Chandra X-Ray Observatory
BI CTI correction: E0102 on S1 Red Chi= 1.57

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Paul Plucinsky

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EPIC Cal October 2006


Chandra X-Ray Observatory
Pollock RGS vs. Flanagan (2004) HETG Line Fluxes
Lin e OVII For OVII Res O VIII Ly- O VIII Ly- Ne IX triplet Ne X Ly- Ne X Ly- Flanagan Flux 13.95 24.38 37.31 6 .3 7 23.18 9 .7 2 2 .0 7
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CXC

Pollock Flux 11.53 27.23 40.65 7 .7 8 21.15 12.70 1 .8 7

(10-4 photons cm-2 s-1) (10-4 photons cm-2 s-1)

Difference +17.3% -1 1 . 7 % -8 . 9 % -1 5 . 9 % +8.8% -3 0 . 7 % +9.7%

Paul Plucinsky

EPIC Cal October 2006


Chandra X-Ray Observatory
O VIII Ly and Ne X Ly Normalization Results

CXC

·
·

Data sets fit independently, O and Ne line complexes are free to vary as a group SMC NH=5.65x1020 cm-2, Bremsstrahlung kT=0.95 keV
Instrumen t ACIS S3 (node 1) ACIS S3 (node 0) O VIII Ly Norm (x 10-3 photons cm-2 s) 6.58 [6.44,6.94] 6.92 [6.79,7.36] 6.14 [6.09,6.19] 6.42 [6.35,6.53] Ne X Ly Norm (x 10-3 photons cm-2 s) 1.80 [1.73,1.88] 1.77 [1.69,1.84] 1.74 [1.72,1.76] 1.71 [1.68,1.73] Red 1.27 1.48 2.69 2.51
2

OBSID 3545 [90% CL] 6765 [90% CL]

DOF 95 93 279 92

0135720801 pn [90% CL] 0135720601 MOS1 [90% CL]

· Ne X Ly a normalizations agree within ~6.0% for ACIS, pn, & MOS1

· Early S3 and MOS1 agree within ~2.0% for O
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VIII Ly normalizations

· Most recent S3 and pn disgree by ~18.0% for O VIII Ly normalizations
Paul Plucinsky

EPIC Cal October 2006


Chandra X-Ray Observatory
Let's Agree on a Model !!!!!!!
Purpose: to improve the low-energy response model of ACIS, MOS and pn CCD instruments

CXC

1 2 3 4 5 6

) ) ) ) ) )

RGS and HETG agree on flux of bright lines RGS and HETG compromise on existence of weak lines RGS and HETG agree on widths for the lines Select a continuum model and absorption HETG team must analyze second epoch observations of E0102 Fit ACIS, MOS, and pn with the same model

Paul Plucinsky

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EPIC Cal October 2006